scholarly journals 59 Cygni: A Tilted ϕ Persei like System

2000 ◽  
Vol 175 ◽  
pp. 581-584 ◽  
Author(s):  
Th. Rivinius ◽  
S. Štefl

AbstractThe binarity of 59 Cygni was confirmed and orbital parameters from the radial velocity curve of the primary derived. The observed emission variability resembles the one of ɸ Per in quite some detail, suggesting a similar nature of the companion: a hot, compact star.

2016 ◽  
Vol 12 (S329) ◽  
pp. 402-402 ◽  
Author(s):  
E. Gosset ◽  
L. Mahy ◽  
Y. Damerdji ◽  
C. Nitschelm ◽  
H. Sana ◽  
...  

AbstractWe present here a modern study of the radial velocity curve and of the photometric light curve of the very interesting supergiant O7.5If + O9I(f) binary system HD 166734. The physical parameters of the stars and the orbital parameters are carefully determined. We also perform the analysis of the observed X-ray light curve of this colliding-wind binary.


2019 ◽  
Vol 491 (4) ◽  
pp. 5489-5497 ◽  
Author(s):  
Oleg Yu Malkov

ABSTRACT Semidetached eclipsing systems provide a unique opportunity to derive the basic properties of interacting binaries. The goal of this work is to collect and to make use of data on semidetached systems with available light and radial velocity curve solutions. I have compiled the most comprehensive list to date, of 119 semidetached double-lined eclipsing binaries, containing the orbital parameters and physical parameters of the components. I consider the classification of semidetached binaries and discuss gaps between various classes in the Hertzspung–Russell diagram. I list systems with component parameters that are inverted and briefly discuss their evolutionary state.


2012 ◽  
Vol 45 (1) ◽  
pp. 1-6 ◽  
Author(s):  
Kamal Ghaderi ◽  
Ali Pirkhedri ◽  
Touba Rostami ◽  
Salem Khodamoradi ◽  
Hedayat Fatahi

1985 ◽  
Vol 87 ◽  
pp. 109-115
Author(s):  
P.W. Hill ◽  
C.S. Jeffery

AbstractNew radial velocity data for the pulsating extreme helium star V652 Her (BD+13°3224) have been obtained with a time resolution of 100 s. High frequency structure in the radial velocity curve is detected, and a comparison with previous data suggests that the detailed shape of the velocity curve is variable. The data imply that the effective surface gravity must increase by a factor of 4 at minimum radius.


1988 ◽  
Vol 100 ◽  
pp. 371 ◽  
Author(s):  
Thaddeus F. Worek ◽  
Eugene R. Zizka ◽  
Merle W. King ◽  
Joost H. Kiewiet de Jonge

1997 ◽  
Vol 123 (2) ◽  
pp. 209-218 ◽  
Author(s):  
R. Duemmler ◽  
I. V. Ilyin ◽  
I. Tuominen

2004 ◽  
Vol 194 ◽  
pp. 269-269 ◽  
Author(s):  
V. V. Neustroev ◽  
S. V. Zharikov ◽  
A. Medvedev ◽  
A. Shearer

We present preliminary results of new spectroscopic observations of dwarf nova BZ UMa in quiescence. Fifty medium resolution spectra allow us to reproduce the radial velocity curve from the Hα emission line. We confirm that BZ UMa shows extremely unusual emission lines profiles, Unlike the classical single or the double-peaked profiles usually observed in spectra of dwarf novae, emission lines of BZ UMa consist of at least five peaks.


Author(s):  
P. M. Veen ◽  
A. M. Van Genderen ◽  
M. A. W. Verhelfen ◽  
K. A. Van Der Hucht

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